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RobertPincus committed Feb 26, 2025
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<div class="trigger"><a class="page-link" href="/rte-rrtmgp/how-tos/build-and-test.html">How to build and run tests</a><a class="page-link" href="/rte-rrtmgp/">RTE+RRTMGP documentation</a><a class="page-link" href="/rte-rrtmgp/explanations/">Explanations</a><a class="page-link" href="/rte-rrtmgp/tutorials/">Tutorials</a><a class="page-link" href="/rte-rrtmgp/how-tos/">How-to guides</a><a class="page-link" href="/rte-rrtmgp/reference/">Reference (technical documentation)</a></div>
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Expand All @@ -43,13 +43,13 @@ <h1 class="post-title">Explanations</h1>
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<h1 id="explanations-will-live-here">Explanations will live here</h1>
<p>RTE+RRTMGP is a set of codes for computing radiative fluxes in planetary atmospheres. These pages provide a orientation to the code’s architcture.</p>

<h3 id="spectral-discretization">Spectral discretization</h3>
<p>RTE <a href="./rte-solvers.html">computes</a> radiative <a href="./rte-fluxes.html"><em>fluxes</em></a> given values of <a href="./rte-optical-props.html"><em>optical properties</em></a> , <a href="./rte-optical-props.html"><em>source functions</em></a>, and boundary conditions.</p>

<p>The spectral properties of the atmosphere and the source functions depend on electromagnetic wavelength (or frequency or wavenumber). RTE treats this spectral dependence by dividing the spectrum into one or more <em>bands</em>, each of which represents a continuous set of wavelengths/frequencies. Bands may be further sub-divided into <em>g-points</em> (the language is borrowed from <em>k</em>-distributions). Each <em>g</em>-point is treated as a independent psudo-monchromatic calculation but there is no inherent mapping between <em>g</em>-points and wavelengths; the sum over <em>g</em>-points is the band-average value.</p>
<p><a href="./rte-optics">RRTMGP computes</a> the optical properties and source functions of the gaseous atmosphere given the distribution of temperature, pressure, and gas concentrations within the atmosphere. RRTMGP includes models for the optics of clouds and aerosols.</p>

<p>The bands defined by RRTMGP cover the full spectrum of radiation emitted by the Sun and Earth: these are <em>broadband</em> calculations. In RRTMGP the bands are continuous so that the ending wavelength of one band is the starting wavelength of the next.</p>
<p>Each of the italicized phrases above corresponds to a class in the Fortran 2003 interface which bundles some combination of code and data.</p>

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<h1 class="post-title">RTE - fluxes</h1>
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<p>RTE solves the radiative transfer equation for each spectral point independently but this detailed information typically isn’t useful. Class <code class="language-plaintext highlighter-rouge">ty_fluxes</code> in module <a href="../reference/rte-fortran-interface/module/mo_fluxes.html">mo_fluxes</a> in the RTE library provides a way to reduce the highly-detailed information based on precisely what the user needs. Class <code class="language-plaintext highlighter-rouge">ty_fluxes_broadband</code> provides an example implementation that reports broadband flux i.e. the sum over all spectral points at all levels.</p>

<h1 id="fluxes-interface">Fluxes interface</h1>

<p><a href="https://earth-system-radiation.github.io/rte-rrtmgp/reference/rte-fortran-interface/type/ty_fluxes.html">ty_fluxes</a> is an abstract class that defines <a href="../reference/rte-fortran-interface/type/ty_fluxes.html">two interfaces</a> defining type-bound functions. Function <code class="language-plaintext highlighter-rouge">reduce()</code> is called within the RTE solvers. The input arguments include the spectrally-resolved fluxes up and down (and, optically, the direct-beam flux) and the spectral discretization. Logical function <code class="language-plaintext highlighter-rouge">are_desired()</code> is called by RTE to check if the results of a calculation will be used.</p>

<p>Class <code class="language-plaintext highlighter-rouge">ty_fluxes</code> is abstract; it defines only the interfaces to these routines. Implementation is deferred to user classes that extend this class.</p>

<h1 id="broadband-fluxes">Broadband fluxes</h1>

<p>Class <a href="../reference/rte-fortran-interface/type/ty_fluxes_broadband.html">ty_fluxes_broadband</a> in the same <a href="../reference/rte-fortran-interface/module/mo_fluxes.html">module</a> provides an example of how to extend <code class="language-plaintext highlighter-rouge">ty_fluxes</code>. This class reports broadband values i.e. the sum over every element in the spectral dimensions. The class contains <a href="../reference/rte-fortran-interface/type/ty_fluxes_broadband.html">four data fields</a>. Before calling one of the RTE solvers with this class as output, users either allocate one or more of these output fields or point to an existing array. The fields must have the same number of columns and layers as the problem being solved. In class <code class="language-plaintext highlighter-rouge">ty_fluxes_broadband</code> logical function `are_desired()`` returns true if one or more of the data fields points to storage and false otherwise.</p>

<h1 id="other-extensions">Other extensions</h1>

<p>Class <code class="language-plaintext highlighter-rouge">ty_fluxes_byband</code> in subdirectory <code class="language-plaintext highlighter-rouge">extensions/</code> provides another example that makes use of the spectral discretization information.</p>

<p>It’s useful to extend the class when particular subsets of fluxes, such as photosynthetically-active radiation at the surface, are required.</p>

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<p>RTE+RRTMGP is a set of codes for computing radiative fluxes in planetary atmospheres. RRTMGP uses a k-distribution to provide an optical description (absorption and possibly Rayleigh optical depth) of the gaseous atmosphere, along with the relevant source functions, on a pre-determined spectral grid given temperatures, pressures, and gas concentration. RTE computes fluxes given spectrally-resolved optical descriptions and source functions.</p>
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